Cosmological Simulations: Successes & Tensions of ɅCDM
|
|
- Elijah Houston
- 5 years ago
- Views:
Transcription
1 Cosmological Simulations: Successes & Tensions of ɅCDM Volker Springel Large scale predictions Small scale predictions Challenges for ɅCDM from non-linear structure formation PASCOS 2011 Conference Cambridge, July 2011
2 Want to bridge 13.6 billion years of cosmological evolution Sun
3 Want to bridge 13.6 billion years of cosmological evolution Mathematical Bridge in Cambridge Sun Rumored to be built by Isaac Newton... without nuts and bolts
4 Currently the fastest supercomputers carry out about ~1 Petaflop, which are one thousand billion floating point operations per second JUGENE IN JUELICH
5
6 Why are cosmological simulations of structure formation useful for studying the dark universe? Simulations are the theoretical tool of choice for calculations in the non-linear regime. They connect the (simple) cosmological initial conditions with the (complex) present-day universe. Predictions from N-body simulations: Abundance of objects (as a function of mass and time) Their spatial distribution Internal structure of halos (e.g. density profiles, spin) Mean formation epochs Merger rates Detailed dark matter distribution on large and fairly small scales Galaxy formation models Gravitational lensing Baryonic acoustic oscillations in the matter distribution Integrated Sachs-Wolfe effect Dark matter annihilation rate Morphology of large-scale structure ( cosmic web )...
7 Simulations provide accurate measurements for halo abundance as a function of time CONVERGENCE RESULTS FOR HALO ABUNDANCE Boylan-Kolchin, Springel, White, et al. (2009)
8 Simulated and observed largescale structure in the galaxy distribution MOCK PIE DIAGRAMS COMPARED TO SDSS, 2DFGRS, AND CFA-2 Springel et al. (2006)
9 The two-point correlation function of galaxies in the Millennium run is a very good power law GALAXY TWO-POINT FUNCTION COMPARED WITH 2dFGRS
10 The galaxy distribution is biased with respect to the mass distribution GALAXY AND MASS CLUSTERING AT DIFFERENT EPOCHS evolves little in time evolves strongly in time
11 The large-scale clustering pattern of halos and galaxies is already imprinted on the initial conditions TIME EVOLUTION OF THE MATTER AND GALAXY DISTRIBUTION
12 The baryonic wiggles remain visible in the galaxy distribution down to low redshift and may serve as a "standard ruler" to constrain dark energy DARK MATTER AND GALAXY POWER SPECTRA FROM THE MILLENNIUM SIMULATION IN THE REGION OF THE WIGGLES Springel et al. (2005)
13 Large volume simulations are needed for ongoing and future surveys GOALS FOR A MILLENNIUM-XXL CALCULATION Science goals Impact of galaxy physics on BAO/growth factor measurements Realistic mock catalogs for Pan-STARRS, SDSS-III/BOSS, BigBOSS, etc. Exploring galaxy physics in different cosmologies Integrated Sachs-Wolfe effect Clustering up to ~500 Mpc/h, universality of halo bias and mass function, rare events, environmental effects, first quasars, etc. Desired simulation characteristics Box-Size: > 3000 Mpc/h Particle mass: < ~ 6 x 109 M /h Particle number: > 300 billion particles
14 Millennium-XXL 303 billion particles Largest N-body simulation ever
15 Millennium-XXL was successfully executed on JUROPA in 2010 PARAMETERS OF FINAL RUN ~ 303 billion particles 3000 Mpc/h box, Millennium cosmology cores: 3072 MPI-task / 4 threads (70% of Juropa) FFT mesh 86 trillion force calculations Cost: 2.7 million CPU hours (~300 years), corresponding to 9.3 days wallclock time (including FOF+SUBFIND) Peak memory usage: 29 TB (105 bytes/particle) 700 million halos at z=0 (44% of particles) About 25 billion (sub)halos in merger trees Largest cluster has 9 x 1015 M Size of a full snapshot: ~10 TB More than 120 TB stored for science JUROPA Jülich Forschungszentrum
16 M-II Millennium MXXL
17 Are the presently known high-mass clusters still consistent with ΛCDM? CLUSTER MASS FOR GIVEN ABUNDANCE AS A FUNCTION OF TIME Detection of one violating cluster would invalidate ΛCDM XMMU J SPT-CL J Holz & Perlmutter (2010) argued XMMU J to be inconsistent with ΛCDM at 3σ Boyle, Jiminez & Verde (2010) argue that σ8 would have to be ~4σ higher to accommodate massive clusters. Suggest nongaussian ICs as a solution.
18 Massive clusters are not homogenous and are often fairly perturbed systems MASSIVE CLUSTERS AT Z = 0.32 Snapshot z= most massive clusters according to M200 M = [2.5 4] x 1015 Msun/h
19
20 Diversity in the Extreme THE MOST MASSIVE AND RAREST CLUSTERS FOLLOW THE SCALING RELATIONS EXPECTED FROM MORE ABUNDANT SMALLER SYSTEMS So far reported massive clusters not in conflict with ΛCDM (yet)
21 NASA Press Release Aug 21, 2006: 1E : NASA Finds Direct Proof of Dark Matter
22 Fitting the density jump in the X-ray surface brightness profile allows a measurement of the shock's Mach number X-RAY SURFACE BRIGHTNESS PROFILE Markevitch et al. (2006) shock strength: M = 3.0 ± 0.4 shock velocity: vs = 4700 km/s Usually, shock velocity has been identified with velocity of the bullet.
23 How rare is the bullet cluster? DISTRIBUTION OF VELOCITIES OF THE MOST MASSIVE SUBSTRUCTURE IN THE MILLENNIUM RUN Hayashi & White (2006) Adopted mass model from Clowe et al. (2004): NFW-Halo with: M200 = 2.96 x 1015 M R200 = 2.25 Mpc V200 = 2380 km/sec Vshock = 4500 km/sec Vsub/Vshock = 1.9 chance: 10-2 But, revised data from Clowe et al. (2006) and Markevitch el al. (2006): M200 = 1.5 x 1015 M V200 = 1680 km/sec Vshock = 4740 km/sec Vsub/Vshock = 2.8 chance: 10-7
24 Observed X-ray map compared with simulation images of a standard zero-energy orbit merger SIMULATED X-RAY MAP COMPARED TO OBSERVATION Candra 500 ks image bullet cluster simulation Springel & Farrar (2007)
25 The model also matches the observed temperature and mass profiles COMPARISON OF SIMULATED TEMPERATURE AND MASS PROFILE WITH OBSERVATIONS Data from Markevitch et al. (2006) Data from Bradac et al. (2006)
26 Despite a shock speed of ~4500 km/s, the bullet moves considerably slower VELOCITIES AND POSITIONS OF MAIN BULLET CLUSTER FEATURES AS A FUNCTION OF TIME Shock speed: 4500 km/s Pre-shock infall: km/s Shock speed relative to bullet: -800 km/s Speed of bullet: 2600 km/s
27 Models with a fifth force in the dark sector can speed up the bullet, but seem not required to match the bullet system SPEED OF THE BULLET IN FIFTH FORCE MERGERS (proposed by Farrar & Rosen 2006) = 1.0 vb = 3800 km/s = 1.0, rs = 4 Mpc = 0.3, rs = 4 Mpc = 1. 0 = 0.3 vb = 3010 km/s =0 vb = 2600 km/s
28 Small-scale dark matter structure
29
30 Zooming in on dark matter halos reveals a huge abundance of dark matter substructure DARK MATTER DISTRIBUTION IN A MILKY WAY SIZED HALO AT DIFFERENT RESOLUTION
31 Spherically averaged density profiles of dark matter halos have a nearly universal shape DENSITY PROFILE AS A FUNCTION OF RADIUS Fundamental importance for: Rotation curve of galaxies Internal structure of galaxy clusters Gravitational lensing DM annihilation Galaxy mergers
32 Our simulations allow us to study the convergence of subhalo density profiles SPHERICALLY AVERAGED DENSITY PROFILES IN THE AQ-A HALO AT DIFFERENT RESOLUTION
33 A long standing issue in galaxy formation theory: The shapes of the CDM halo mass function and the galaxy luminosity function are very different THE OBSERVED LF COMPARED TO THE SHAPE OF THE CDM HALO MASS FUNCTION van den Bosch et al. (2004)
34 Taken at face value, the number of luminous satellites in the Milky Way is much smaller than the number of dark matter lumps THE SATELLITE PROBLEM Moore et al. (1999)
35 GIMIC Project, Theuns et al. (2009) Hydrodynamical simulations aim to predict: Morphology of galaxies Fate of the diffuse gas, WHIM, metal enrichment X-ray atmospheres in halos Turbulence in halos and accretion shocks Large-scale regulation of star formation in galaxies through feedback processes from stars and black holes Transport processes (e.g. conduction) Radiative transfer Dynamical transformations (e.g. ram-pressure stripping) Magnetic fields
36 Current cosmological hydrodynamic simulations have severe trouble to explain the low galaxy formation efficiency required for ΛCDM GALAXY FORMATION EFFICIENCY AS A FUNCTION OF HALO MASS Guo, White & Boylan-Kolchin (2010) Sawala & White (2010)
37 Relatively dense massive subhalos are predicted that apparently cannot host any of the luminuous satellites of the Milky Way THE PUZZLING DARKNESS OF SOME OF THE LARGE DARK MATTER SATELLITES Boylan-Kolchin, Bullock & Kaplinghat (2011)
38 Warm dark matter models also reduce the number of Milky Way satellites substantially for 1 kev there are still enough SATELLITE ABUNDANCE AS A FUNCTION OF DM PARTICLE MASS Maccio & Fontanot (2010)
39 The radial distribution of substructures is strongly antibiased relative to all dark matter, and independent of subhalo mass RADIAL SUBSTRUCTURE DISTRIBUTION IN Aq-A-1 Most subhalos are at large radii, subhalos are more effectively destroyed near the centre Subhalos are far from the Sun see also Diemand et al. (2007, 2008)
40 The subhalo abundance per unit halo mass is surprisingly uniform VELOCITY FUNCTION IN OUR DIFFERENT HALOS
41 The cumulative mass fraction in resolved substructures reaches about 12-13%, we expect up to ~18% down to the thermal limit FRACTION OF MASS IN SUBSTRUCTURES AS A FUNCTION OF MASS LIMIT thermal limit
42 Dark matter annihilation predictions
43 Dark matter could be self-annihilating, in which case the presence of subhalos should boost the expected flux THE ANNIHILATION SIGNAL DUE TO SUBSTRUCTURES Annihilation flux: Particle physics Astrophysics Luminosity of a halo with maximum circular velocity Vc(rmax)= Vmax: NFW-Profile: α = -1.4 Profile: Einasto-Profile: Moore-Profile:
44 The dark matter annihilation flux is boosted significantly by dark matter substructures EXTRAPOLATED ALL-SKY MAP OF THE DM ANNIHILATION FLUX FROM THE MILKY WAY L ρ2 dv Aq-A-2
45 Dark matter annihilation can be best discovered with an optimal filter against a bright background THE SIGNAL-TO-NOISE FOR DETECTION WITH AN OPTIMAL FILTER signal The optimal filter is proportional to the signal background noise The background dominates, then: Main halo's smooth component: Subhalo's smooth component: S/N ~ F / θ S/N ~ L / rh d Sub-substructure of a subhalo:
46 Detectability of different annihilation emission components in the Milky Way S/N for detecting subhalos in units of that for the main halo 30 highest S/N objects, assuming the use of optimal filters sub-subhalos main subhalos known satellites Highest S/N subhalos have 1% of S/N of main halo Highest S/N subhalos have 10 times S/N of known satellites Substructure of subhalos has no influence on detectability
47 But what about other nearby structures, like galaxy clusters? High resolution Phoenix project Gao et al. (2011)
48 The nearest massive galaxy clusters are attractive targets for annihilation detection COMPARISON OF SIGNAL-TO-NOISE FOR DETECTION OF NEARBY SOURCES
49 The Millennium-II simulation can be used to construct full backwards lightcones of the expected gamma-ray annihilation background SIMULATION BOX STACKING AND EXTRAPOLATION OF HALO PROPERTIES Zavala, Springel & Boylan-Kolchin (2010)
50 Thin redshift slices of the gamma-ray background reveal cosmic large-scale structure A PARTIAL MAP AT ENERGY 10 GEV NEAR Z~0
51 In the complete coadded map, individual structures vanish in the high background level except for very near halos THE FULL BACKGROUND MAP OUT TO REDSHIFT Z = 10
52 The full-sky maps can be used to extract direct predictions for the properties of the background ENERGY SPECTRUM OF THE BACKGROUND
53 Coupled dark energy models get around some of the fine-tuning problems associated with dark energy, but introduce non-trivial modifications of long-range forces COUPLED DARK ENERGY IN THE NEWTONIAN LIMIT Basic equations: Wetterich (1995) Amendola (2000) Expanding to linear order in Newtonian gauge: Varying dark matter particle mass term extra friction term Modified gravitational interaction Implemented by Baldi et al. (2009) in the GADGET-3 code
54 The numerical implementation accurately matches the linear theory on large-scales and predicts shallower halo profiles on small scales SOME RESULTS FOR COUPLED DARK ENERGY SIMULATIONS Baldi et al. (2009) Interestingly, the above results is opposite to earlier numerical findings: Baldi et al. (2009) Maccio et al. (2004)
55 Summary points Direct numerical simulations have become indispensable for studying the non-linear growth of structures in CDM cosmologies. Current numerical techniques allow high-resolution simulations with an unprecedented dynamic range. One presently reaches N>1011, with a dynamic range of in 3D. The future observation of a sufficiently massive cluster may easily rule out the ΛCDM model. The predicted satellite population may still be in tension with the observations. Understanding galaxy formation physics remains a serious challenge in ΛCDM, both at the faint and the bright end. Dark matter annihilation radiation should be more easily detectable from Coma or Fornax compared with nearby satellites. Simulations of structure formation in modified gravity still in their infancy, but they promise to put powerful constraints on the viable model space.
Simulations of Cosmic Structure Formation
Simulations of Cosmic Structure Formation Volker Springel The role of simulations in cosmology High-resolution N-body simulations Millennium XXL Hydrodynamic simulations and recent results for galaxy formation
More informationSimulating non-linear structure formation in dark energy cosmologies
Simulating non-linear structure formation in dark energy cosmologies Volker Springel Distribution of WIMPS in the Galaxy Early Dark Energy Models (Margherita Grossi) Coupled Dark Energy (Marco Baldi) Fifth
More informationDwarf Galaxies as Cosmological Probes
Dwarf Galaxies as Cosmological Probes Julio F. Navarro The Ursa Minor dwarf spheroidal First Light First Light The Planck Satellite The Cosmological Paradigm The Clustering of Dark Matter The Millennium
More informationPrinceton December 2009 The fine-scale structure of dark matter halos
Princeton December 2009 The fine-scale structure of dark matter halos Simon White Max Planck Institute for Astrophysics The dark matter structure of CDM halos A rich galaxy cluster halo Springel et al
More informationThe Formation and Evolution of Galaxy Clusters
IAU Joint Discussion # 10 Sydney, July, 2003 The Formation and Evolution of Galaxy Clusters Simon D.M. White Max Planck Institute for Astrophysics The WMAP of the whole CMB sky Bennett et al 2003 > 105
More informationStructure and substructure in dark matter halos
Satellites and Tidal Streams ING IAC joint Conference La Palma, May 2003 Structure and substructure in dark matter halos Simon D.M. White Max Planck Institute for Astrophysics 500 kpc A CDM Milky Way Does
More informationStructure formation in the concordance cosmology
Structure formation in the Universe, Chamonix, May 2007 Structure formation in the concordance cosmology Simon White Max Planck Institute for Astrophysics WMAP3 team WMAP3 team WMAP3 team WMAP3 team In
More informationThe Los Cabos Lectures
January 2009 The Los Cabos Lectures Dark Matter Halos: 2 Simon White Max Planck Institute for Astrophysics EPS statistics for the standard ΛCDM cosmology Millennium Simulation cosmology: Ωm = 0.25, ΩΛ
More informationTHE BOLSHOI COSMOLOGICAL SIMULATIONS AND THEIR IMPLICATIONS
GALAXY FORMATION - Durham -18 July 2011 THE BOLSHOI COSMOLOGICAL SIMULATIONS AND THEIR IMPLICATIONS JOEL PRIMACK, UCSC ΛCDM Cosmological Parameters for Bolshoi and BigBolshoi Halo Mass Function is 10x
More informationA unified multi-wavelength model of galaxy formation. Carlton Baugh Institute for Computational Cosmology
A unified multi-wavelength model of galaxy formation Carlton Baugh Institute for Computational Cosmology M81 Angel Lopez Sanchez A unified multi-wavelength model of galaxy formation Lacey et al. 2015 arxiv:1509.08473
More informationThe Millennium-XXL Project: Simulating the Galaxy Population of dark Energy Universes
The Millennium-XXL Project: Simulating the Galaxy Population of dark Energy Universes 20 Modern cosmology as encoded in the leading!cdm model confronts astronomers with two major puzzles. One is that the
More informationDark matter from cosmological probes
PLANCK 2014 Ferrara Dark matter from cosmological probes Simon White Max Planck Institute for Astrophysics Dark matter was discovered in the Coma Cluster by Zwicky (1933) Fritz Zwicky Abell 2218 Corbelli
More informationPiTP Summer School 2009
PiTP Summer School 2009 Plan for my lectures Volker Springel Lecture 1 Basics of collisionless dynamics and the N-body approach Lecture 2 Gravitational solvers suitable for collisionless dynamics, parallelization
More informationModelling the galaxy population
Modelling the galaxy population Simon White Max Planck Institut für Astrophysik IAU 277 Ouagadougou 1 The standard model reproduces -- the linear initial conditions -- IGM structure during galaxy formation
More information2. What are the largest objects that could have formed so far? 3. How do the cosmological parameters influence structure formation?
Einführung in die beobachtungsorientierte Kosmologie I / Introduction to observational Cosmology I LMU WS 2009/10 Rene Fassbender, MPE Tel: 30000-3319, rfassben@mpe.mpg.de 1. Cosmological Principles, Newtonian
More informationConstraints on dark matter annihilation cross section with the Fornax cluster
DM Workshop@UT Austin May 7, 2012 Constraints on dark matter annihilation cross section with the Fornax cluster Shin ichiro Ando University of Amsterdam Ando & Nagai, arxiv:1201.0753 [astro-ph.he] Galaxy
More informationFormation and growth of galaxies in the young Universe: progress & challenges
Obergurgl. April 2014 Formation and growth of galaxies in the young Universe: progress & challenges Simon White Max Planck Institute for Astrophysics Ly α forest spectra and small-scale initial structure
More informationThe Millennium Simulation: cosmic evolution in a supercomputer. Simon White Max Planck Institute for Astrophysics
The Millennium Simulation: cosmic evolution in a supercomputer Simon White Max Planck Institute for Astrophysics The COBE satellite (1989-1993) Two instruments made maps of the whole sky in microwaves
More informationCosmological Puzzles: Dwarf Galaxies and the Local Group
Cosmological Puzzles: Dwarf Galaxies and the Local Group Julio F. Navarro Dark-matter-only simulations have highlighted a number of cosmological puzzles Local Group puzzles Missing satellites problem Satellite
More informationThe Los Cabos Lectures
January 2009 The Los Cabos Lectures Dark Matter Halos: 3 Simon White Max Planck Institute for Astrophysics Shapes of halo equidensity surfaces Group Jing & Suto 2002 Galaxy δ 100 2500 6250 Shapes of halo
More informationSome like it warm. Andrea V. Macciò
Some like it warm Andrea V. Macciò MPIA - Heidelberg D. Aderhalden, A. Schneider, B. Moore (Zurich), F. Fontanot (HITS), A. Dutton, J. Herpich, G. Stinson (MPIA), X. Kang (PMO) CDM problems, hence WDM
More informationImpact of substructures on predictions of dark matter annihilation signals
Impact of substructures on predictions of dark matter annihilation signals Julien Lavalle Institute & Dept. of Theoretical Physics, Madrid Aut. Univ. & CSIC DESY Theory Astroparticle, Hamburg 16 V 2011
More informationActive Galaxies and Galactic Structure Lecture 22 April 18th
Active Galaxies and Galactic Structure Lecture 22 April 18th FINAL Wednesday 5/9/2018 6-8 pm 100 questions, with ~20-30% based on material covered since test 3. Do not miss the final! Extra Credit: Thursday
More informationAdvanced Topics on Astrophysics: Lectures on dark matter
Advanced Topics on Astrophysics: Lectures on dark matter Jesús Zavala Franco e-mail: jzavalaf@uwaterloo.ca UW, Department of Physics and Astronomy, office: PHY 208C, ext. 38400 Perimeter Institute for
More informationThe Iguaçu Lectures. Nonlinear Structure Formation: The growth of galaxies and larger scale structures
April 2006 The Iguaçu Lectures Nonlinear Structure Formation: The growth of galaxies and larger scale structures Simon White Max Planck Institute for Astrophysics z = 0 Dark Matter ROT EVOL Cluster structure
More informationCurrent status of the ΛCDM structure formation model. Simon White Max Planck Institut für Astrophysik
Current status of the ΛCDM structure formation model Simon White Max Planck Institut für Astrophysik The idea that DM might be a neutral, weakly interacting particle took off around 1980, following a measurement
More informationHunting for dark matter in the forest (astrophysical constraints on warm dark matter)
Hunting for dark matter in the forest (astrophysical constraints on warm dark matter) ICC, Durham! with the Eagle collaboration: J Schaye (Leiden), R Crain (Liverpool), R Bower, C Frenk, & M Schaller (ICC)
More informationDark Matter. Jaan Einasto Tartu Observatory and ICRANet 16 December Saturday, December 15, 12
Dark Matter Jaan Einasto Tartu Observatory and ICRANet 16 December 2012 Local Dark Matter: invisible matter in the Galaxy in Solar vicinity Global Dark Matter: invisible matter surrounding galaxies Global
More informationVeilleux! see MBW ! 23! 24!
Veilleux! see MBW 10.4.3! 23! 24! MBW pg 488-491! 25! But simple closed-box model works well for bulge of Milky Way! Outflow and/or accretion is needed to explain!!!metallicity distribution of stars in
More informationhalo formation in peaks halo bias if halos are formed without regard to the underlying density, then δn h n h halo bias in simulations
Physics 463, Spring 07 Bias, the Halo Model & Halo Occupation Statistics Lecture 8 Halo Bias the matter distribution is highly clustered. halos form at the peaks of this distribution 3 2 1 0 halo formation
More informationGravitational Lensing of the Largest Scales
What is dark matter? Good question. How do we answer it? Gravitational lensing! Gravitational lensing is fantastic Why Clusters of Galaxies Because they are cool!! Studying empirical properties of dark
More informationASTRON 449: Stellar (Galactic) Dynamics. Fall 2014
ASTRON 449: Stellar (Galactic) Dynamics Fall 2014 In this course, we will cover the basic phenomenology of galaxies (including dark matter halos, stars clusters, nuclear black holes) theoretical tools
More informationFeedback, AGN and galaxy formation. Debora Sijacki
Feedback, AGN and galaxy formation Debora Sijacki Formation of black hole seeds: the big picture Planck data, 2013 (new results 2015) Formation of black hole seeds: the big picture CMB black body spectrum
More informationThe imprint of the initial conditions on large-scale structure
Stars, Planets and Galaxies 2018 Harnack House, Berlin The imprint of the initial conditions on large-scale structure Simon White Max Planck Institute for Astrophysics The Planck map of TCMB the initial
More informationDark Matter Substructure and their associated Galaxies. Frank C. van den Bosch (MPIA)
Dark Matter Substructure and their associated Galaxies Frank C. van den Bosch (MPIA) Outline PART I: The Subhalo Mass Function (van den Bosch, Tormen & Giocoli, 2005) PART II: Statistical Properties of
More informationInsights into galaxy formation from dwarf galaxies
Potsdam, August 2014 Insights into galaxy formation from dwarf galaxies Simon White Max Planck Institute for Astrophysics Planck CMB map: the IC's for structure formation Planck CMB map: the IC's for structure
More informationThe fine-scale structure of dark matter halos
COSMO11, Porto, August 2011 The fine-scale structure of dark matter halos Simon White Max-Planck-Institute for Astrophysics COSMO11, Porto, August 2011 Mark Vogelsberger The fine-scale structure of dark
More informationBullet Cluster: A Challenge to ΛCDM Cosmology
Bullet Cluster: A Challenge to ΛCDM Cosmology Eiichiro Komatsu (Texas Cosmology Center, UT Austin) Fundamental Physics and Large-scale Structure, Perimeter Institute April 29, 2010 1 This talk is based
More informationTesla Jeltema. Assistant Professor, Department of Physics. Observational Cosmology and Astroparticle Physics
Tesla Jeltema Assistant Professor, Department of Physics Observational Cosmology and Astroparticle Physics Research Program Research theme: using the evolution of large-scale structure to reveal the fundamental
More informationStructure Formation and Evolution"
Structure Formation and Evolution" From this (Δρ/ρ ~ 10-6 )! to this! (Δρ/ρ ~ 10 +2 )! to this! (Δρ/ρ ~ 10 +6 )! How Long Does It Take?" The (dissipationless) gravitational collapse timescale is on the
More informationSome useful spherically symmetric profiles used to model galaxies
Some useful spherically symmetric profiles used to model galaxies de Vaucouleurs R 1/4 law for ellipticals and bulges A good fit to the light profile of many ellipticals and bulges: (constant such that
More informationGaia Revue des Exigences préliminaires 1
Gaia Revue des Exigences préliminaires 1 Global top questions 1. Which stars form and have been formed where? - Star formation history of the inner disk - Location and number of spiral arms - Extent of
More informationA brief history of cosmological ideas
A brief history of cosmological ideas Cosmology: Science concerned with the origin and evolution of the universe, using the laws of physics. Cosmological principle: Our place in the universe is not special
More informationA. Thermal radiation from a massive star cluster. B. Emission lines from hot gas C. 21 cm from hydrogen D. Synchrotron radiation from a black hole
ASTR 1040 Accel Astro: Stars & Galaxies Prof. Juri Toomre TA: Nicholas Nelson Lecture 26 Thur 14 Apr 2011 zeus.colorado.edu/astr1040-toomre toomre HST Abell 2218 Reading clicker what makes the light? What
More informationWhat can we learn from galaxy clustering measurements II. Shaun Cole Institute for Computational Cosmology Durham University
What can we learn from galaxy clustering measurements II Shaun Cole Institute for Computational Cosmology Durham University Introduction Galaxy clustering has two distinct uses: 1. Large scale tracers
More informationStar systems like our Milky Way. Galaxies
Galaxies Star systems like our Milky Way Galaxies Contain a few thousand to tens of billions of stars,as well as varying amounts of gas and dust Large variety of shapes and sizes Gas and Dust in
More informationThe Galaxy Dark Matter Connection
The Galaxy Dark Matter Connection constraining cosmology & galaxy formation Frank C. van den Bosch (MPIA) Collaborators: Houjun Mo (UMass), Xiaohu Yang (SHAO) Marcello Cacciato, Surhud More, Simone Weinmann
More informationLARGE QUASAR GROUPS. Kevin Rahill Astrophysics
LARGE QUASAR GROUPS Kevin Rahill Astrophysics QUASARS Quasi-stellar Radio Sources Subset of Active Galactic Nuclei AGNs are compact and extremely luminous regions at the center of galaxies Identified as
More informationAGN in hierarchical galaxy formation models
AGN in hierarchical galaxy formation models Nikos Fanidakis and C.M. Baugh, R.G. Bower, S. Cole, C. Done, C. S. Frenk Physics of Galactic Nuclei, Ringberg Castle, June 18, 2009 Outline Brief introduction
More informationGalaxy population simulations
Aspen, February 2014 Galaxy population simulations Simon White Max Planck Institute for Astrophysics semi-analytic simulations provide a tool... To explore the statistics and interactions of the many processes
More informationDark Matter & Dark Energy. Astronomy 1101
Dark Matter & Dark Energy Astronomy 1101 Key Ideas: Dark Matter Matter we cannot see directly with light Detected only by its gravity (possible future direct detection in the lab) Most of the matter in
More informationFormation and evolution of CDM halos and their substructure
Formation and evolution of CDM halos and their substructure 1) cold dark matter and structures on all scales 2) via lactea, z=0 results 3) subhalo evolution Jürg Diemand UC Santa Cruz 4) DM annihilation
More informationAGN feedback and its influence on massive galaxy evolution
AGN feedback and its influence on massive galaxy evolution Darren Croton (University of California Berkeley) Simon White, Volker Springel, et al. (MPA) DEEP2 & AEGIS collaborations (Berkeley & everywhere
More informationReview of Lecture 15 3/17/10. Lecture 15: Dark Matter and the Cosmic Web (plus Gamma Ray Bursts) Prof. Tom Megeath
Lecture 15: Dark Matter and the Cosmic Web (plus Gamma Ray Bursts) Prof. Tom Megeath A2020 Disk Component: stars of all ages, many gas clouds Review of Lecture 15 Spheroidal Component: bulge & halo, old
More informationThe halo-galaxy connection KITP, May 2017` Assembly bias. Simon White Max Planck Institute for Astrophysics
The halo-galaxy connection KITP, May 2017` Assembly bias Simon White Max Planck Institute for Astrophysics Halo clustering depends on formation history Gao, Springel & White 2005 The 20% of halos with
More informationWhere are the missing baryons? Craig Hogan SLAC Summer Institute 2007
Where are the missing baryons? Craig Hogan SLAC Summer Institute 2007 Reasons to care Concordance of many measures of baryon number (BBN, CMB,.) Evolution of our personal baryons (galaxies, stars, planets,
More informationThe Alexandria Lectures
March 2006 The Alexandria Lectures Numerical Cosmology: Recreating the Universe in a Supercomputer Simon White Max Planck Institute for Astrophysics The Three-fold Way to Astrophysical Truth OBSERVATION
More informationWeak Gravitational Lensing
Weak Gravitational Lensing Sofia Sivertsson October 2006 1 General properties of weak lensing. Gravitational lensing is due to the fact that light bends in a gravitational field, in the same fashion as
More informationGalaxy clusters. Dept. of Physics of Complex Systems April 6, 2018
Galaxy clusters László Dobos Dept. of Physics of Complex Systems dobos@complex.elte.hu É 5.60 April 6, 2018 Satellite galaxies Large galaxies are surrounded by orbiting dwarfs approx. 14-16 satellites
More informationGamma-rays from Earth-Size dark-matter halos
Gamma-rays from Earth-Size dark-matter halos Tomoaki Ishiyama, Jun Makino, Toshikazu Ebisuzaki, and Veniamin Berezinsky Presentation by: JM Bottom line Microhalos (mass earth mass) do survive to the present
More informationThe Milky Way Galaxy. Some thoughts. How big is it? What does it look like? How did it end up this way? What is it made up of?
Some thoughts The Milky Way Galaxy How big is it? What does it look like? How did it end up this way? What is it made up of? Does it change 2 3 4 5 This is not a constant zoom The Milky Way Almost everything
More informationChapter 17. Active Galaxies and Supermassive Black Holes
Chapter 17 Active Galaxies and Supermassive Black Holes Guidepost In the last few chapters, you have explored our own and other galaxies, and you are ready to stretch your scientific imagination and study
More informationDark Matter ASTR 2120 Sarazin. Bullet Cluster of Galaxies - Dark Matter Lab
Dark Matter ASTR 2120 Sarazin Bullet Cluster of Galaxies - Dark Matter Lab Mergers: Test of Dark Matter vs. Modified Gravity Gas behind DM Galaxies DM = location of gravity Gas = location of most baryons
More informationThe Caustic Technique An overview
The An overview Ana Laura Serra Torino, July 30, 2010 Why the mass of? Small scales assumption of dynamical equilibrium Mass distribution on intermediate scales (1 10 Mpc/h) Large scales small over densities
More informationCOSMOLOGY PHYS 30392 OBSERVING THE UNIVERSE Part I Giampaolo Pisano - Jodrell Bank Centre for Astrophysics The University of Manchester - January 2013 http://www.jb.man.ac.uk/~gp/ giampaolo.pisano@manchester.ac.uk
More informationCross-Correlation of Cosmic Shear and Extragalactic Gamma-ray Background
Cross-Correlation of Cosmic Shear and Extragalactic Gamma-ray Background Masato Shirasaki (Univ. of Tokyo) with Shunsaku Horiuchi (UCI), Naoki Yoshida (Univ. of Tokyo, IPMU) Extragalactic Gamma-Ray Background
More informationThe galaxy population in cold and warm dark matter cosmologies
The galaxy population in cold and warm dark matter cosmologies Lan Wang National Astronomical Observatories, CAS Collaborators: Violeta Gonzalez-Perez, Lizhi Xie, Andrew Cooper, Carlos Frenk, Liang Gao,
More informationAstro-2: History of the Universe. Lecture 5; April
Astro-2: History of the Universe Lecture 5; April 23 2013 Previously.. On Astro-2 Galaxies do not live in isolation but in larger structures, called groups, clusters, or superclusters This is called the
More informationNumerical Cosmology & Galaxy Formation
Numerical Cosmology & Galaxy Formation Lecture 13: Example simulations Isolated galaxies, mergers & zooms Benjamin Moster 1 Outline of the lecture course Lecture 1: Motivation & Historical Overview Lecture
More informationIsotropy and Homogeneity
Cosmic inventory Isotropy and Homogeneity On large scales the Universe is isotropic (looks the same in all directions) and homogeneity (the same average density at all locations. This is determined from
More informationPHYSICAL COSMOLOGY & COMPLEXITY
PHYSICAL COSMOLOGY & COMPLEXITY The Quest for the Invisible Universe Pier Stefano Corasaniti CNRS & Observatoire de Paris OUTLINE Epistemological Perspective: Invisible Universe and Cosmic Structure Formation:
More informationWhere to Look for Dark Matter Weirdness
Where to Look for Dark Matter Weirdness Dark Matter in Southern California (DaMaSC) - II James Bullock UC Irvine Garrison-Kimmel, Oñorbe et al. Collaborators Mike Boylan-Kolchin U. Maryland Miguel Rocha
More informationThe rise of galaxy surveys and mocks (DESI progress and challenges) Shaun Cole Institute for Computational Cosmology, Durham University, UK
The rise of galaxy surveys and mocks (DESI progress and challenges) Shaun Cole Institute for Computational Cosmology, Durham University, UK Mock Santiago Welcome to Mock Santiago The goal of this workshop
More informationmodified gravity? Chaire Galaxies et Cosmologie XENON1T Abel & Kaehler
Dark matter or modified gravity? Chaire Galaxies et Cosmologie Françoise Combes 11 December, 2017 XENON1T Abel & Kaehler Why modified gravity? CDM models beautifully account for LSS, CMB, galaxy formation
More informationLarge-scale structure as a probe of dark energy. David Parkinson University of Sussex, UK
Large-scale structure as a probe of dark energy David Parkinson University of Sussex, UK Question Who was the greatest actor to portray James Bond in the 007 movies? a) Sean Connery b) George Lasenby c)
More informationThe Cosmological Redshift. Cepheid Variables. Hubble s Diagram
SOME NEGATIVE EFFECTS OF THE EXPANSION OF THE UNIVERSE. Lecture 22 Hubble s Law and the Large Scale Structure of the Universe PRS: According to modern ideas and observations, what can be said about the
More informationThe Formation and Evolution of Galaxy Clusters
Distant Clusters of Galaxies Ringberg, October, 2005 The Formation and Evolution of Galaxy Clusters Simon D.M. White Max Planck Institute for Astrophysics Bennett et al 2003 > 105 near-independent 5 temperature
More informationOther Galaxy Types. Active Galaxies. A diagram of an active galaxy, showing the primary components. Active Galaxies
Other Galaxy Types Active Galaxies Active Galaxies Seyfert galaxies Radio galaxies Quasars Origin??? Different in appearance Produce huge amount of energy Similar mechanism a Galactic mass black hole at
More informationClusters and groups of galaxies: internal structure and dynamics
Clusters and groups of galaxies: internal structure and dynamics Strong constraints on cosmological theories and on the nature of dark matter can be obtained from the study of cluster masses, mass distribution,
More informationA.Klypin. Dark Matter Halos
A.Klypin Dark Matter Halos 1 Major codes: GADET N-body Hydro Cooling/Heating/SF Metal enrichment Radiative transfer Multistepping/Multiple masses Springel, SDM White PKDGRAV - GASOLINE ART ENZO Quinn,
More informationAST541 Lecture Notes: Galaxy Formation Dec, 2016
AST541 Lecture Notes: Galaxy Formation Dec, 2016 GalaxyFormation 1 The final topic is galaxy evolution. This is where galaxy meets cosmology. I will argue that while galaxy formation have to be understood
More informationFeedback and Galaxy Formation
Heating and Cooling in Galaxies and Clusters Garching August 2006 Feedback and Galaxy Formation Simon White Max Planck Institute for Astrophysics Cluster assembly in ΛCDM Gao et al 2004 'Concordance'
More informationProbing Dark Matter Halos with Satellite Kinematics & Weak Lensing
Probing Dark Matter Halos with & Weak Lensing Frank C. van den Bosch (MPIA) Collaborators: Surhud More, Marcello Cacciato UMass, August 2008 Probing Dark Matter Halos - p. 1/35 Galaxy Formation in a Nutshell
More informationCosmic Rays in Galaxy Clusters: Simulations and Perspectives
Cosmic Rays in Galaxy Clusters: Simulations and Perspectives 1 in collaboration with Volker Springel 2, Torsten Enßlin 2 1 Canadian Institute for Theoretical Astrophysics, Canada 2 Max-Planck Institute
More informationSmoothed Particle Hydrodynamics (SPH) a meshfree particle method for astrophysics *
Smoothed Particle Hydrodynamics (SPH) a meshfree particle method for astrophysics * Supplement 3: Example simulations using SPH and advanced graphics David Hobbs Lund Observatory ASTM17 Galaxy collision
More informationMoore et al Kenney et al. 2004
Moore et al. 1996 Kenney et al. 2004 (i) Interaction with other cluster members and/or with the cluster potential (ii) Interactions with the hot gas that permeates massive galaxy systems. The influence
More informationAnalyzing the CMB Brightness Fluctuations. Position of first peak measures curvature universe is flat
Analyzing the CMB Brightness Fluctuations (predicted) 1 st rarefaction Power = Average ( / ) 2 of clouds of given size scale 1 st compression 2 nd compression (deg) Fourier analyze WMAP image: Measures
More informationDurham Lightcones: Synthetic galaxy survey catalogues from GALFORM. Jo Woodward, Alex Merson, Peder Norberg, Carlton Baugh, John Helly
Durham Lightcones: Synthetic galaxy survey catalogues from GALFORM Jo Woodward, Alex Merson, Peder Norberg, Carlton Baugh, John Helly Outline 1. How are the lightcone mocks constructed? 2. What mocks are
More informationFormation and cosmic evolution of supermassive black holes. Debora Sijacki
Formation and cosmic evolution of supermassive black holes Debora Sijacki Summer school: Black Holes at all scales Ioannina, Greece, Sept 16-19, 2013 Lecture 1: - formation of black hole seeds - low mass
More informationASTR 200 : Lecture 25. Galaxies: internal and cluster dynamics
ASTR 200 : Lecture 25 Galaxies: internal and cluster dynamics 1 Galaxy interactions Isolated galaxies are often spirals One can find small galaxy `groups' (like the Local group) with only a few large spiral
More informationCLUMPY: A public code for γ-ray and ν signals from dark matter structures.
CLUMPY: A public code for γ-ray and ν signals from dark matter structures. Moritz Hütten, DESY Zeuthen for the CLUMPY developers: Vincent Bonnivard, Moritz Hütten, Emmanuel Nezri, Aldée Charbonnier, Céline
More informationBackground Picture: Millennium Simulation (MPA); Spectrum-Roentgen-Gamma satellite (P. Predehl 2011)
By Collaborators Alex Kolodzig (MPA) Marat Gilfanov (MPA,IKI), Gert Hütsi (MPA), Rashid Sunyaev (MPA,IKI) Publications Kolodzig et al. 2013b, A&A, 558, 90 (ArXiv : 1305.0819) Hüsti et al. 2014, submitted
More informationThe cosmic distance scale
The cosmic distance scale Distance information is often crucial to understand the physics of astrophysical objects. This requires knowing the basic properties of such an object, like its size, its environment,
More informationThe Galaxy Dark Matter Connection
The Galaxy Dark Matter Connection constraining cosmology & galaxy formation Frank C. van den Bosch (MPIA) Collaborators: Houjun Mo (UMass), Xiaohu Yang (SHAO) Marcello Cacciato, Surhud More, Simone Weinmann
More informationMoment of beginning of space-time about 13.7 billion years ago. The time at which all the material and energy in the expanding Universe was coincident
Big Bang Moment of beginning of space-time about 13.7 billion years ago The time at which all the material and energy in the expanding Universe was coincident Only moment in the history of the Universe
More informationGamma-ray background anisotropy from Galactic dark matter substructure
Gamma-ray background anisotropy from Galactic dark matter substructure Shin ichiro Ando (TAPIR, Caltech) Ando, arxiv:0903.4685 [astro-ph.co] 1. Introduction Dark matter annihilation and substructure Dark
More informationCosmic ray feedback in hydrodynamical simulations. simulations of galaxy and structure formation
Cosmic ray feedback in hydrodynamical simulations of galaxy and structure formation Canadian Institute for Theoretical Astrophysics, Toronto April, 13 26 / Workshop Dark halos, UBC Vancouver Outline 1
More informationClusters of Galaxies Groups: Clusters poor rich Superclusters:
Clusters of Galaxies Galaxies are not randomly strewn throughout space. Instead the majority belong to groups and clusters of galaxies. In these structures, galaxies are bound gravitationally and orbit
More informationTHE MAGIC TELESCOPES. Major Atmospheric Gamma Imaging Cherenkov Telescopes
THE MAGIC TELESCOPES Observatorio del Roque de los Muchachos, La Palma (2200 m a.s.l.) System of two 17 m Cherenkov Telescopes for VHE γ-ray astronomy MAGIC-I operational since 2004, Stereo system since
More informationThe Formation of Galaxies: connecting theory to data
Venice, October 2003 The Formation of Galaxies: connecting theory to data Simon D.M. White Max Planck Institute for Astrophysics The Emergence of the Cosmic Initial Conditions > 105 independent ~ 5 measurements
More information